DOCSLIB.ORG

Redalyc.SEARCH for GAMMA-RAY EMISSION from THE

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Redalyc.SEARCH for GAMMA-RAY EMISSION from THE Revista Mexicana de Astronomía y Astrofísica ISSN: 0185-1101 [email protected] Instituto de Astronomía México García López, R. J.; the MAGIC Collaboration SEARCH FOR GAMMA-RAY EMISSION FROM THE SUPERNOVA REMNANT IC 443 WITH THE MAGIC TELESCOPE Revista Mexicana de Astronomía y Astrofísica, vol. 35, junio, 2009, pp. 62-63 Instituto de Astronomía Distrito Federal, México Available in: http://www.redalyc.org/articulo.oa?id=57115758021 How to cite Complete issue Scientific Information System More information about this article Network of Scientific Journals from Latin America, the Caribbean, Spain and Portugal Journal's homepage in redalyc.org Non-profit academic project, developed under the open access initiative RevMexAA (Serie de Conferencias), 35, 62{63 (2009) SEARCH FOR GAMMA-RAY EMISSION FROM THE SUPERNOVA REMNANT IC 443 WITH THE MAGIC TELESCOPE R. J. Garc´ıa L´opez1,2 on behalf of the MAGIC Collaboration3 RESUMEN Observaciones de muy alta energ´ıa (TeV) de remanentes de supernova y, en particular, de aqu´ellos que parecen estar relacionados f´ısicamente con fuentes detectadas por el sat´elite EGRET constituyen un objetivo primario para el telescopio MAGIC. Su resoluci´on espacial y sensibilidad pueden usarse para verificar el principal meca- nismo responsable de la producci´on de fotones de alta energ´ıa en los alrededores de un remanente de supernova. Siguiendo los resultados de un an´alisis sistem´atico reciente del entorno molecular localizado en la vecindad de todas los remanentes detectados por EGRET, se seleccion´o el remanente IC 443 para su observaci´on con MAGIC. Aqu´ı se describe brevemente la estrategia observacional que dio lugar a la detecci´on de una nueva fuente de rayos gamma de muy alta energ´ıa: MAGIC J0616+225. ABSTRACT TeV observations of Supernova remnants (SNRs) and, in particular, of SNRs which appear to be physically related to EGRET sources are a prime target for the MAGIC telescope. MAGIC's spatial resolution and sensi- tivity can probe the main mechanism responsible for producing high energy photons in the SNR neighbourhood. Based on a recent systematical analysis of the molecular environment of the vicinity of all SNR-EGRET source pairs, the IC 443 remnant was chosen for observations with MAGIC. We briefly describe the observational strategy which provided the detection of a new very-high energy gamma-ray source: MAGIC J0616+225. Key Words: gamma rays: observations | ISM: individual (IC 443, MAGIC J0616+225) | supernova remnants 1. INTRODUCTION: THE COSMIC RAYS Where this mechanism could be working? A clue: PROBLEM total cosmic rays power amounts to ∼ 10% of a- verage supernova power. However, direct observa- Cosmic rays constitute a continuous flow of re- tion of cosmic rays in the line of sight of a supernova lativistic particles, mainly protons and alpha parti- remnant (SNR) does not provide information of their cles (99%). Their energy spctrum is a power-law / Ed. G. Magris, Bruzual, & L. Carigi − : source because, being charged particles, they are a- E 2 2, which spans many orders of magnitude indi- ffected by Galactic magnetic fields. On the other cating a non-thermal origin. Their energy density hand, gamma-ray production is expected in the same equals that of \normal" stellar light reaching the environment and carries the location information. Earth. For E > 108 eV their chemical composition resembles that of solar system, but it is very different There are two main production mechanisms isotopically. for gamma-rays: electron acceleration by mag- Up to 1015 eV their origin is mainly Galactic, but netic fields, with X-ray synchrotron production and what are the acceleration mechanisms operating in gamma-ray production by inverse Compton with a / −2:6 the Galaxy? Currently, there is only one known to spectrum E ; and accelerated protons interac- ting with a nucleus producing pions which decay in © 2009: Instituto de Astronomía, UNAM - 12th IAU Regional Latin American Meeting of Astronomy be efficient enough: the first-order Fermi mechanism. / −2:2 In this scenario, particles crossing a shock front can gamma-rays with a spectrum E . These last be scattered randomly inside and outside the front ones can be used to probe mechanisms for particle gaining momentum and, finally, escape with a higher acceleration. velocity. This mechanisms produces a flux spectrum Why IC 443 was selected? Following the system- −α proportional to E with α ∼> 2. atical analysis of Torres et al. (2003), in which all positional coincidences between SNRs and unidenti- 1Instituto de Astrof´ısica de Canarias, C/ V´ıa L´actea s/n, fied γ-ray sources listed in the Third EGRET Catalog 38205 La Laguna, Tenerife, Spain ([email protected]). 2 at low Galactic latitudes are discussed on a case by Departamento de Astrof´ısica, Universidad de La Laguna, case basis, it was found that one of the most po- Av. Astrof´ısico Francisco S´anchez s/n, 38206 La Laguna, Tenerife, Spain. werful unidentified sources is positionally coincident 3http://wwwmagic.mppmu.mpg.de/. with this SNR. It is a symmetric shell-type SNR 62 VHE GAMMA RADIATION FROM IC 443 OBSERVED WITH MAGIC 63 a b Fig. 1. (a) Distribution of excess γ-ray candidate events as a function of the squared angular distance from the excess center of the source MAGIC J0616+225 (points), compared to the expected distribution for a point like source (solid line) corresponding to the MAGIC point spread function (PSF). (b) VHE γ-ray spectrum of this source compared to the spectrum of the Crab Nebula as measured by MAGIC. Both figures are taken from Albert et al. (2007). with 450 diameter, at ∼ 1:5 kpc, detected also in for December 2006{January 2007 (only 29 useful). radio and X rays (presence of accelerated electrons). Its analysis confirmed the previous hypothesis. Furthermore, there is a large amount of molecular As a result, a new VHE gamma-ray source was 4 mass (∼ 10 M ) consistent with the distance to the discovered: MAGIC J0616+225 (Figure 1a). It ap- SNR (possibility of pion production). Also, a 1720 pears to be a point like source, spatially coincident MHz maser emission is detected: shocked gas, thus with a high density molecular cloud and maser emis- acceleration expected. And, finally, a pulsar wind sion, but marginally coincident with the EGRET nebula (PWN) is located near the SNR shell. On unidentified source (probably unrelated to it). It the other hand, only upper limits to the very-high seems to be also unrelated to the PWN located Ed. G. Magris, Bruzual, & L. Carigi energy (VHE) γ-ray emission had been established closely. previously for this source. Figure 1b shows that its spectrum is / E−3:10:3, which is far from that expected for pure proton ac- 2. OBSERVATIONS AND RESULTS celeration. Currently, a good model for this source is The MAGIC (Major Atmospheric Gamma Ima- lacking. A detailed analysis of the multi-wavelength ging Cerenkov) telescope is a 17m diameter atmos- data available, as well as a deeper discussion of this pheric imaging Cherenkov detector, with a mirror result can be found in the paper by Albert et al. surface of 236 m2 and photomultiplier tubes of op- (2007). timal efficiency. With the accent on best light col- IN MEMORIAM. Maurizio Panniello, PhD stu- lection, it can detect cosmic gamma-rays at a low e- © 2009: Instituto de Astronomía, UNAM - 12th IAU Regional Latin American Meeting of Astronomy dent at the Instituto de Astrof´ısica de Canarias and nergy threshold (70 GeV). It is located at the Roque a very active member of the MAGIC Collaboration, de los Muchachos Observatory in the island of La carried out part of the 2007 observations that allo- Palma (Canary Islands). A second twin telescope is wed this discovery. Very sadly, he suffered an acci- under construction and will start its operations at dent inside a cave at the North of the island of Tene- the end of 2008. rife in February of that year and passed away. This A first observing run of IC 443 was carried out work is dedicated to his memory. in December 2005{January 2006 (10 hours), and its analysis showed evidence of signal (3σ excess on a REFERENCES 2 2 0.05 deg region out of a 2.25 deg map). This excess Albert, J., et al. 2007, ApJ, 664, L87 was supposed to be associated with a γ-ray source Torres, D. F., Romero, G. E., Dame, T. M., Combi, J. A., and additional 40 hours of observation were approved & Butt, Y. M. 2003, Phys. Rep., 382, 303.
Load more

Recommended publications
  • Filter Performance Comparisons for Some Common Nebulae
    Filter Performance Comparisons For Some Common Nebulae By Dave Knisely Light Pollution and various “nebula” filters have been around since the late 1970’s, and amateurs have been using them ever since to bring out detail (and even some objects) which were difficult to impossible to see before in modest apertures. When I started using them in the early 1980’s, specific information about which filter might work on a given object (or even whether certain filters were useful at all) was often hard to come by. Even those accounts that were available often had incomplete or inaccurate information. Getting some observational experience with the Lumicon line of filters helped, but there were still some unanswered questions. I wondered how the various filters would rank on- average against each other for a large number of objects, and whether there was a “best overall” filter. In particular, I also wondered if the much-maligned H-Beta filter was useful on more objects than the two or three targets most often mentioned in publications. In the summer of 1999, I decided to begin some more comprehensive observations to try and answer these questions and determine how to best use these filters overall. I formulated a basic survey covering a moderate number of emission and planetary nebulae to obtain some statistics on filter performance to try to address the following questions: 1. How do the various filter types compare as to what (on average) they show on a given nebula? 2. Is there one overall “best” nebula filter which will work on the largest number of objects? 3.
    [Show full text]
  • Supernova Shocks in Molecular Clouds: Velocity Distribution of Molecular Hydrogen William T
    Draft version September 6, 2019 Typeset using LATEX preprint2 style in AASTeX63 Supernova Shocks in Molecular Clouds: Velocity Distribution of Molecular Hydrogen William T. Reach,1 Le Ngoc Tram,1 Matthew Richter,2 Antoine Gusdorf,3 Curtis DeWitt,1 1Universities Space Research Association, MS 232-11, Moffett Field, CA 94035, USA 2University of California, Davis, CA USA 3Observatoire de Paris, Ecole´ normale sup´erieure, Sorbonne Universit´e,CNRS, LERMA, 75005 Paris, France ABSTRACT Supernovae from core-collapse of massive stars drive shocks into the molecular clouds from which the stars formed. Such shocks affect future star formation from the molecu- lar clouds, and the fast-moving, dense gas with compressed magnetic fields is associated with enhanced cosmic rays. This paper presents new theoretical modeling, using the Paris-Durham shock model, and new observations at high spectral resolution, using the Stratospheric Observatory for Infrared Astronomy (SOFIA), of the H2 S(5) pure rota- tional line from molecular shocks in the supernova remnant IC 443. We generate MHD models for non-steady-state shocks driven by the pressure of the IC 443 blast wave into gas of densities 103 to 105 cm−3. We present the first detailed derivation of the shape of the velocity profile for emission from H2 lines behind such shocks, taking into account the shock age, preshock density, and magnetic field. For preshock densities 103{105 −3 cm , the H2 emission arises from layers that extend 0.01{0.0003 pc behind the shock, respectively. The predicted shifts of line centers, and the line widths, of the H2 lines range from 20{2, and 30{4 km s−1, respectively.
    [Show full text]
  • How to Make $1000 with Your Telescope! – 4 Stargazers' Diary
    Fort Worth Astronomical Society (Est. 1949) February 2010 : Astronomical League Member Club Calendar – 2 Opportunities & The Sky this Month – 3 How to Make $1000 with your Telescope! – 4 Astronaut Sally Ride to speak at UTA – 4 Aurgia the Charioteer – 5 Stargazers’ Diary – 6 Bode’s Galaxy by Steve Tuttle 1 February 2010 Sunday Monday Tuesday Wednesday Thursday Friday Saturday 1 2 3 4 5 6 Algol at Minima Last Qtr Moon Æ 5:48 am 11:07 pm Top ten binocular deep-sky objects for February: M35, M41, M46, M47, M50, M93, NGC 2244, NGC 2264, NGC 2301, NGC 2360 Top ten deep-sky objects for February: M35, M41, M46, M47, M50, M93, NGC 2261, NGC 2362, NGC 2392, NGC 2403 7 8 9 10 11 12 13 Algol at Minima Morning sports a Moon at Apogee New Moon Æ super thin crescent (252,612 miles) 8:51 am 7:56 pm Moon 8:00 pm 3RF Star Party Make use of the New Moon Weekend for . better viewing at the Dark Sky Site See Notes Below New Moon New Moon Weekend Weekend 14 15 16 17 18 19 20 Presidents Day 3RF Star Party Valentine’s Day FWAS Traveler’s Guide Meeting to the Planets UTA’s Maverick Clyde Tombaugh Ranger 8 returns Normal Room premiers on Speakers Series discovered Pluto photographs and NatGeo 7pm Sally Ride “Fat Tuesday” Ash Wednesday 80 years ago. impacts Moon. 21 22 23 24 25 26 27 Algol at Minima First Qtr Moon Moon at Perigee Å (222,345 miles) 6:42 pm 12:52 am 4 pm {Low in the NW) Algol at Minima Æ 9:43 pm Challenge binary star for month: 15 Lyncis (Lynx) Challenge deep-sky object for month: IC 443 (Gemini) Notable carbon star for month: BL Orionis (Orion) 28 Notes: Full Moon Look for a very thin waning crescent moon perched just above and slightly right of tiny Mercury on the morning of 10:38 pm Feb.
    [Show full text]
  • A Multispectral Analysis of the Northeastern Shell of IC 443
    MNRAS 000,1–13 (2019) Preprint 13 August 2019 Compiled using MNRAS LATEX style file v3.0 A multispectral analysis of the northeastern shell of IC 443 Alexandre Alarie,1;2;3 Laurent Drissen,2;3 1 Instituto de Astronomía, Universidad National Autónoma de México, Apdo. Postal 70264, 04510 Mexico D.F., Mexico 2 Département de physique, de génie physique et d’optique, Université Laval, Québec, QC, G1V 0A6, Canada 3 Centre de Recherche en Astrophysique du Québec 13 August 2019 ABSTRACT We have carried out optical observations of the north-eastern part of the supernova remnant IC 443 using the CFHT imaging spectrograph SITELLE. The observations consist of three multispectral cubes covering an 110 ×110 area allowing the investigation of both the spatial and spectral variation of 9 emission lines : [O II] ll3726+3729, [O III] ll4959,5007, Hb, Ha, [N II] ll6548,6583 and [S II] ll6716,6731. Extinction measurement from the Ha/Hb shows significant variation across the observed region with E(B-V) = 0.8-1.1. Electron density measurements using [S II] lines indicate densities ranging from 100 up to 2500 cm−3. Models computed with the shock modelling code MAPPINGS are presented and compared with the observations. A combination of complete shock model and truncated ones are required in order to explain the observed spectrum. The shock velocities found in IC 443 are between 20 and 150 km s−1 with 75 km s−1 being the most prominent velocity. The pre-shock number density varies from 20 to 60 cm−3. A single set of abundances close to solar values combined with varying shock parameters (shock velocity, pre-shock density and shock age) are sufficient to explain the great variation of lines intensities observed in IC 443.
    [Show full text]
  • List of Bright Nebulae Primary I.D. Alternate I.D. Nickname
    List of Bright Nebulae Alternate Primary I.D. Nickname I.D. NGC 281 IC 1590 Pac Man Neb LBN 619 Sh 2-183 IC 59, IC 63 Sh2-285 Gamma Cas Nebula Sh 2-185 NGC 896 LBN 645 IC 1795, IC 1805 Melotte 15 Heart Nebula IC 848 Soul Nebula/Baby Nebula vdB14 BD+59 660 NGC 1333 Embryo Neb vdB15 BD+58 607 GK-N1901 MCG+7-8-22 Nova Persei 1901 DG 19 IC 348 LBN 758 vdB 20 Electra Neb. vdB21 BD+23 516 Maia Nebula vdB22 BD+23 522 Merope Neb. vdB23 BD+23 541 Alcyone Neb. IC 353 NGC 1499 California Nebula NGC 1491 Fossil Footprint Neb IC 360 LBN 786 NGC 1554-55 Hind’s Nebula -Struve’s Lost Nebula LBN 896 Sh 2-210 NGC 1579 Northern Trifid Nebula NGC 1624 G156.2+05.7 G160.9+02.6 IC 2118 Witch Head Nebula LBN 991 LBN 945 IC 405 Caldwell 31 Flaming Star Nebula NGC 1931 LBN 1001 NGC 1952 M 1 Crab Nebula Sh 2-264 Lambda Orionis N NGC 1973, 1975, Running Man Nebula 1977 NGC 1976, 1982 M 42, M 43 Orion Nebula NGC 1990 Epsilon Orionis Neb NGC 1999 Rubber Stamp Neb NGC 2070 Caldwell 103 Tarantula Nebula Sh2-240 Simeis 147 IC 425 IC 434 Horsehead Nebula (surrounds dark nebula) Sh 2-218 LBN 962 NGC 2023-24 Flame Nebula LBN 1010 NGC 2068, 2071 M 78 SH 2 276 Barnard’s Loop NGC 2149 NGC 2174 Monkey Head Nebula IC 2162 Ced 72 IC 443 LBN 844 Jellyfish Nebula Sh2-249 IC 2169 Ced 78 NGC Caldwell 49 Rosette Nebula 2237,38,39,2246 LBN 943 Sh 2-280 SNR205.6- G205.5+00.5 Monoceros Nebula 00.1 NGC 2261 Caldwell 46 Hubble’s Var.
    [Show full text]
  • X-Ray and Gamma-Ray Studies of Particle Acceleration in Supernova Remnants
    X-Ray and Gamma-Ray Studies of Particle Acceleration in Supernova Remnants Takaaki Tanaka (KIPAC, Stanford University) Fermi LAT results presented on behalf of the Fermi LAT collaboration Teraelectronvolt Astronomy 37 SNRs = Cosmic-Ray Sources? Supernova remnants have been thought to be accelerating cosmic rays up to the knee (PeV) thorough the diffusive shock acceleration mechanism Synchrotron X-rays and TeV gamma rays from SNRs = Evidence of acceleration up to TeV energies SN 1006 Chandra H.E.S.S. 30′ Figure 6: Four SNRs imaged in (dominantly) non-thermal X-rays (left) and resolved in VHE γ-rays with H.E.S.S. (right). a) RX J1713.7 3946 with 1–3 keV data from ASCA (Uchiyama, Takahashi & Aharonian −2002), b) RX J0852.0 4622 with ROSAT (1.3–2.4 keV) (Aschenbach 1998), c) RCW86 with− 2–4 keV data from XMM-Newton (Vinketal. 2006) d) SN 1006 with Chandra archive data (0.5–10 keV). The H.E.S.S. data are taken from Aharonian et al. (2006b, 2007d), Aharonian & etal.(2008), Naumann-Godo & et al. (2006). The white scale bars are 0.5◦ long. Suzaku (XIS + HXD) Results ① Suzaku has been probing electrons accelerated in SNRs through XIS + HXD measurements of synchrotron X-rays ① RX J1713.7–3946 (Takahashi+ 2008; Tanaka+ 2008) ② Tycho (Tamagawa+ 2009) ③ Cassiopeia A (Maeda+ 2009) No. S1] Suzaku Observations of Tycho’s SNR S173 No. 6] Possible keV–TeV Correlation in the Reverse Shock 1223 ② ③ Fig. 8. (a) XIS and PIN spectra fitted with a thermal bremsstrahlung, an srcut model, and GaussianFig. lines.
    [Show full text]
  • The X-Ray Structure and Spectrum of the Pulsar Wind Nebula Surrounding PSR B1853+01 in W44
    The X-ray Structure and Spectrum of the Pulsar Wind Nebula Surrounding PSR B1853+01 in W44 R. Petre, K. D. Kuntz 1 NASA Goddard Space Flight Center, Greenbelt, MD 20771 and R. L. Shelton The Henry A. Rowland Department of Physics and Astronomy, Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218 ABSTRACT We present the result of a Chandra ACIS observation of the pulsar PSR B1853+01 and its associated pulsar wind nebula (PWN), embedded within the supernova remnant W44. A hard band ACIS map cleanly distinguishes the PWN from the thermal emission of W44. The nebula is extended in the north-south direction, with an extent about half that of the radio emission. Morphological differences between the X-ray and radio images are apparent. Spectral fitting reveals a clear difference in spectral index between the hard emission from PSR B1853+01 (F --_ 1.4) and the extended nebula (F --, 2.2). The more accurate values for the X-ray flux and spectral index are used refine estimates for PWN parameters, including magnetic field strength, the average Lorentz factor _ of the particles in the wind, the magnetization parameter a, and the ratio k of electrons to other particles. Subject headings: supernova remnants--ISM:individual(W 44)--X-rays:general 1. Introduction fated, old radio pulsars. Additionally, because of its high proper motion, the pulsar leaves a record The remarkable pulsar wind nebula associated of its evolution embedded in the extended neb- with PSR B1853+01 and embedded in the evolved, ula. A combination of high resolution radio and mixed-morphology supernova remnant W44 is of X-ray observations can potentially disentangle this particular interest for several reasons.
    [Show full text]
  • Dave Knisely's Filter Performance Comparisons for Some Common Nebulae Quick Reference
    Dave Knisely's Filter Performance Comparisons For Some Common Nebulae Quick Reference Ref Name DEEP-SKY UHC OIII H-BETA Recommendation M1 CRAB NEBULA 3 4 3 0 UHC/DEEP-SKY (H-beta *not* recommended) M8 LAGOON NEBULA 3 5 5 2 UHC/OIII M16 EAGLE NEBULA 2 4 4 2 UHC/OIII, but H-BETA hurts the view M17 SWAN (OMEGA) NEBULA 3 4 5 1 OIII/UHC (H-BETA not recommended) M20 TRIFID NEBULA 2 4 3 4 UHC/H-BETA M27 DUMBELL NEBULA 3 5 4 1 UHC (OIII also useful in showing some inner detail, but H-BETA is NOT recommended) M42 GREAT ORION NEBULA 3 5 4 3 UHC/OIII (near-tie) M43 North part of Great Orion Nebula 3 3 2 4 H-BETA (UHC and Deep-Sky also help) M57 RING NEBULA 2 4 4 0 UHC/OIII (H-BETA is NOT recommended!) M76 “MINI-DUMBELL” or BUTTERFLY NEBULA 2 4 3 0 UHC/OIII (H-BETA NOT recommended!) M97 OWL NEBULA 2 4 5 0 OIII/UHC (H-beta *not* recommended) NGC 40 3 3 2 2 DEEP-SKY/UHC (near tie) NGC 246 2 3 4 0 OIII/UHC. (H-Beta *not* recommended) NGC 281 3 4 4 2 UHC/OIII. NGC 604 HII region in galaxy M33 in Triangulum 2 3 4 2 OIII/UHC NGC 896/IC 1795 “Heart” nebula 3 4 4 1 UHC/OIII (H-beta *not* recommended) NGC 1360 2 4 4 0 OIII/UHC (H-beta *not* recommended) NGC 1491 3 5 4 0 UHC/OIII (H-Beta *not* recommended) NGC 1499 CALIFORNIA NEBULA 2 2 1 4 H-BETA NGC 1514 CRYSTAL-BALL NEBULA 2 4 4 0 OIII/UHC (H-Beta NOT recommended) NGC 1999 2 1 1 1 DEEP-SKY NGC 2022 3 4 5 0 OIII/UHC (H-Beta NOT recommended) NGC 2024 FLAME NEBULA 3 3 2 1 DEEP-SKY/UHC (near tie) NGC 2174 2 4 4 0 UHC/OIII (near tie) (H-Beta NOT recommended) NGC 2327 2 3 2 4 H-BETA/UHC NGC 2237-9 ROSETTE NEBULA 2 5 5 1 UHC/OIII NGC 2264 CONE NEBULA 2 3 2 1 UHC (other filters may be more useful in larger apertures) NGC 2359 THOR’S HELMET 2 4 5 0 OIII/UHC (H-Beta *not* recommended) NGC 2346 2 3 3 0 UHC/OIII (near tie) (H-beta *not* recommended) NGC 2438 2 3 4 0 OIII (H-Beta *not* recommended) NGC 2371-2 2 4 4 0 OIII/UHC (near tie) (H-Beta *not* recommended) NGC 2392 ESKIMO NEBULA 2 4 4 0 OIII/UHC.
    [Show full text]
  • Astronomy Magazine 2012 Index Subject Index
    Astronomy Magazine 2012 Index Subject Index A AAR (Adirondack Astronomy Retreat), 2:60 AAS (American Astronomical Society), 5:17 Abell 21 (Medusa Nebula; Sharpless 2-274; PK 205+14), 10:62 Abell 33 (planetary nebula), 10:23 Abell 61 (planetary nebula), 8:72 Abell 81 (IC 1454) (planetary nebula), 12:54 Abell 222 (galaxy cluster), 11:18 Abell 223 (galaxy cluster), 11:18 Abell 520 (galaxy cluster), 10:52 ACT-CL J0102-4915 (El Gordo) (galaxy cluster), 10:33 Adirondack Astronomy Retreat (AAR), 2:60 AF (Astronomy Foundation), 1:14 AKARI infrared observatory, 3:17 The Albuquerque Astronomical Society (TAAS), 6:21 Algol (Beta Persei) (variable star), 11:14 ALMA (Atacama Large Millimeter/submillimeter Array), 2:13, 5:22 Alpha Aquilae (Altair) (star), 8:58–59 Alpha Centauri (star system), possibility of manned travel to, 7:22–27 Alpha Cygni (Deneb) (star), 8:58–59 Alpha Lyrae (Vega) (star), 8:58–59 Alpha Virginis (Spica) (star), 12:71 Altair (Alpha Aquilae) (star), 8:58–59 amateur astronomy clubs, 1:14 websites to create observing charts, 3:61–63 American Astronomical Society (AAS), 5:17 Andromeda Galaxy (M31) aging Sun-like stars in, 5:22 black hole in, 6:17 close pass by Triangulum Galaxy, 10:15 collision with Milky Way, 5:47 dwarf galaxies orbiting, 3:20 Antennae (NGC 4038 and NGC 4039) (colliding galaxies), 10:46 antihydrogen, 7:18 antimatter, energy produced when matter collides with, 3:51 Apollo missions, images taken of landing sites, 1:19 Aristarchus Crater (feature on Moon), 10:60–61 Armstrong, Neil, 12:18 arsenic, found in old star, 9:15
    [Show full text]
  • The Very High Energy Characteristics of Shell-Type Snrs and Pulsar Wind Nebulae at Different Ages
    Journal of Physics: Conference Series PAPER • OPEN ACCESS Related content - Non-Thermal Photon Emission from Shell- The very high energy characteristics of shell-type Type Supernova Remnants Dou Ya-Nan and Zhang Li SNRs and Pulsar Wind Nebulae at different ages - Waveguide CO2 laser with a power per unit length of about 1 W/cm W J Witteman, M Ilieva, B I Ilyukhin et al. To cite this article: V G Sinitsyna et al 2016 J. Phys.: Conf. Ser. 718 052045 - Pulse-periodic YAG laser system with phase conjugation I Yu Anikeev, A A Gordeev, I G Zubarev et al. View the article online for updates and enhancements. This content was downloaded from IP address 131.169.5.251 on 08/02/2019 at 23:15 XIV International Conference on Topics in Astroparticle and Underground Physics (TAUP 2015) IOP Publishing Journal of Physics: Conference Series 718 (2016) 052045 doi:10.1088/1742-6596/718/5/052045 The very high energy characteristics of shell-type SNRs and Pulsar Wind Nebulae at different ages V G Sinitsyna, A Y Alaverdyan, M S Andreeva, K A Balygin, S S Borisov, I A Ivanov, A M Kirichenko, A I Klimov, I P Kozhukhova, R M Mirzafatikhov, N I Moseiko, S I Nikolsky, I E Ostashev, A I Palamarchuk,V Y Sinitsyna, I G Volokh P.N. Lebedev Physical Institute, Leninsky pr. 53, Moscow, Russia E-mail: [email protected] Abstract. The investigation of VHE gamma-ray sources by any methods, including mirror Cherenkov telescopes, touches on the problem of the cosmic ray origin and, accordingly, the role of the Galaxy in their generation.
    [Show full text]
  • Annual Report 2011
    ANNUAL REPORT 2011 ON THE COVER: HEADQUARTERS LOCATION: FY2011 Ace summit operations team Kamuela, Hawai’i, USA Number of Full Time members, from left: Arnold Employees: 115 Matsuda, John Baldwin and MANAGEMENT: Mike Dahler, focus their California Association for Number of Observing attention to removing a Research in Astronomy Astronomers FY2011: 464 single segment from the PARTNER INSTITUTIONS: Number of Keck Science Keck Telescope primary California Institute of Investigations: 400 mirror in the first major step Technology (CIT/Caltech), in the segment recoating Number of Refereed Articles process. University of California (UC), FY2011: 278 National Aeronautics and Fiscal Year begins October 1 BELOW: Space Administration (NASA) The newly commissioned Federal Identification Keck I Laser penetrates the OBSERVATORY DIRECTOR: Number: 95-3972799 night sky from the majestic Taft E. Armandroff landscape of Mauna Kea. DEPUTY DIRECTOR: The laser is part of Keck’s Hilton A. Lewis world leading adaptive optics systems, a technology used to remove the effects of turbulence in Earth’s atmosphere and provides unprecedented image clarity of cosmic targets near and distant. VISION A world in which all humankind is inspired and united by the pursuit of knowledge of the infinite CONTENTS variety and richness of the Universe. Director’s Report . 3 Cosmic Visionaries . 6 Science Highlights . 8 MISSION Finances . 16 To advance the frontiers of astronomy and share Philanthropic Support . .18 our discoveries, inspiring the imagination of all. Reflections . .20 Education & Outreach . .22 Observatory Groundbreaking: 1985 Honors & Recognition . .26 First light Keck I telescope: 1992 Science Bibliography . 28 First light Keck II telescope: 1996 DIRECTOR’s REPORT Taft E.
    [Show full text]
  • 1988Apj. . .335. .215P the Astrophysical Journal, 335:215-238
    .215P The Astrophysical Journal, 335:215-238,1988 December 1 © 1988. The American Astronomical Society. AU rights reserved. Printed in U.S.A. .335. 1988ApJ. A COMPREHENSIVE STUDY OF THE X-RAY STRUCTURE AND SPECTRUM OF IC 443 R. Petre and A. E. Szymkowiak Laboratory for High Energy Astrophysics, NASA/Goddard Space Flight Center F. D. Seward Harvard/Smithsonian Center for Astrophysics AND R. WlLLINGALE Leicester University Received 1986 August 26; accepted 1988 May 31 ABSTRACT We present the results of a comprehensive study of the X-ray emission from the supernova remnant IC 443, using the SSS, IPC, and HRI of the Einstein Observatory and the MED of the HEAO 1 A-2 experiment. We observe a soft X-ray appearance highly atypical of a supernova remnant in the adiabatic phase, with little correlation between X-ray and optical or radio features. The best-fit models of the low-energy X-ray spectrum of the brightest area of the remnant suggest either that the remnant has not yet attained ionization equi- librium or that the X-rays arise in a multiphase medium. Pronounced soft X-ray spectral differences across the remnant are accounted for by variations in absorption by an intervening molecular cloud. Our analysis sug- gests that despite the atypical X-ray appearance, the X-ray emission in IC 443 is probably confined to a thin (0.1 pc) shell. Subject headings: nebulae: individual (IC 443) — nebulae: supernovae — X-rays: sources I. INTRODUCTION compression of shocked gas and the consequent compression Recent detailed studies of individual supernova remnants of ambient magnetic fields and relativistic particles transverse have revealed that few, if any, closely resemble the elegant to the direction of the shock.
    [Show full text]